A Manual of Spherical and Practical Astronomy: Embracing the General Problems of Spherical Astronomy, the Special Applications to Nautical Astronomy, and the Theory and Use of Fixed and Portable Astronomical Instruments, with an Appendix on the Method of Least Squares
J. B. Lippincott & Company, 1863
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aberration accuracy altitude ascension and declination assumed astronomical axis azimuth Bessel celestial sphere centre chronometer clock correction co-ordinates coefficient computed constant Corr corresponding curve deduce denote determine difference of longitude diurnal motion earth eclipse employed Ephemeris epoch equal equations of condition equinox expressed formula geocentric given gives Greenwich Greenwich mean hence horizon horizontal parallax hour angle instant instrument interpolation interval latitude logarithms lunar mean meridian method moon nearly noon nutation obtain place of observation plane pole position precession precision prime vertical probable error proper motion quantity radius reckoned reduced refraction result right ascension semidiameter sextant sidereal solar solar eclipse spherical star star's substitute sun's supposed surface taken temperature term tion transit triangle true longitude vernal equinox whence zenith distance
Seite 172 - The mean value of k' is about 57", which may be employed when a very precise result is not required. Fig. 17. DIP OF THE HORIZON. 121. The dip of the horizon is the angle of depression of the visible sea horizon below the true horizon, arising from the elevation of the eye of the observer above the level of the sea.
Seite 317 - ... more and more diverge from the truth. The methods referred 'to in the preceding articles are, therefore, generally to be preferred. 212. The latitude may also be found from two altitudes by the simple method proposed by Captain SUMNER, for which see Chapter VUL CHAPTER VII. FINDING THE LONGITUDE BY ASTRONOMICAL OBSERVATIONS. 213. THE longitude of a point on the earth's surface is the angle at the pole included between the meridian of the point and some assumed first meridian. The difference of...
Seite 28 - A, and the sides b and c, to find the angle B and the side a. The general relations between these five quantities are [Sph. Trig. Art. 114]* cos a = cos c cos b -\- sin c sin b cos A | sin a cos B = sin c cos b — cos c sin b cos A...
Seite 673 - The squares of the periods of revolution of any two planets are proportional to the cubes of their mean distances from the sun.
Seite 593 - ... the solar parallax.* The transits of Venus will afford a far more accurate determination of this parallax than those of Mercury; for, on account of its greater proximity to the earth, the difference in the duration of the transit at different places will be much greater, and the coefficient of AT in the final equations proportionally great. Although the general method for eclipses may also be extended to the prediction of the transits of the planets (by Art. 322), yet it is more convenient in...
Seite 84 - Avhich we set out. The law of the coefficients in (71) is that the coefficient of any odd difference is obtained from that of the preceding odd difference by introducing two factors, one at the beginning and the other at the end of the line of factors, observing as before that these factors are respectively greater and less by unity than those next to which they are placed; and the coefficients of the even differences are obtained from the next preceding even differences in the same manner. The factors...
Seite 223 - ... the condition that the sun should be near the prime vertical may then be satisfied within a few minutes of noon; and in case the ship's latitude is exactly equal to the declination, it will be satisfied only when the sun is on the meridian in the zenith. In such cases the two equal altitudes may be observed within a few minutes of each other, and all corrections, whether for change of latitude or change of declination, may be disregarded. CHAPTER VI. FINDING THE LATITUDE BY ASTRONOMICAL OBSERVATIONS....
Seite 53 - A sidereal day is the interval of time between two successive upper transits of the vernal equinox over the same meridian.
Seite 71 - ... instant. When the sun is on a meridian in west longitude, the Greenwich apparent time is precisely equal to the longitude, that is, the Gr.
Seite 196 - ... will be fully discussed in Vol. II. It will there be seen, also, that the time may be found from transits over any vertical circle. SECOND METHOD. — BY EQUAL ALTITUDES. 139. (A.) Equal altitudes of a fixed star. — The time of the meridian transit of a fixed star is the mean between the two times when it is at the same altitude east and west of the meridian; so that the observation of these two times is a convenient substitute for that of the meridian passage when a transit instrument is not...